Análisis espectroscópico de la estrella Be k Draconis y la estrella cefeida T vulpécula

Abstract

Spectroscopy is one of the most useful tools in astrophysics, since it allows to know fundamental, such as chemical composition, temperature, rotational speed, etc. stellar physical properties In this context, it is known that Be stars have a circumstellar disk of gas generated by the high speed of rotation of these stars. This disc is reflected in the stellar spectrum using hydrogen emission lines that vary in intensity over time. Also, the Cepheid variables, of great importance in determining extragalactic distances, presenting the relationship between the pulsation period and luminosity caused by completely different to that of Be stars mechanisms. In this work were reduced, calibrated and analyzed the spectra of the star Be  Draconis and Cepheid T Vulpecula, obtained with the Boller & Chivens spectrograph San Pedro Martir Astronomical Observatory (Institute of Astronomy at UNAM, Mexico). The process of reduction and calibration of the spectra was performed using IRAF (Image Reduction and Analysis Facility) software. These spectra were used to obtain the chemical composition of the atmospheres of these stars, spectral type and effective temperature. Also, both spectra in order to gain a better understanding of developmental differences between the two types of objects from a view spectroscopic compared.